叠合星系团弱透镜分析中星系团三轴性的引入

Zhuowen Zhang, Hao-Yi Wu, Yuanyuan Zhang, J. Frieman
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引用次数: 1

摘要

星系团的计数提供了对宇宙学的高精度探测,但对系统误差的控制将决定测量的准确性。利用Buzzard模拟,我们量化了一个这样的系统,即使用redMaPPer光学星团发现算法识别的星团的三轴性分布,该算法用于暗能量调查第一年(DES Y1)星团宇宙学分析。我们测试了redMaPPer的选择是否会对集群的形状和方向产生偏差,发现它只会对方向产生偏差,优先选择长轴沿视线方向的集群。将丰富度-质量关系建模为对数线性,发现对数丰富度振幅ln (A)从最低方向向最高方向增强,显著性为14σ,而丰富度-质量斜率和本然散射的方向依赖性最小。我们还发现,在不同方向箱中,星团相关暗晕的弱透镜剪切轮廓比类似于一个“瓶颈”形状,可以用柯西函数量化。我们测试了方向与星系团宇宙学中另外两个主要的系统论——错定和投影——的相关性,发现零相关。从我们的模板中预测得到的质量偏差证实了DES Y1的发现,即三轴性是星系团宇宙学中偏差的主要来源。然而,偏差的丰度依赖性证实了三轴性并不能完全解决DES Y1星系团宇宙学与其他探测器之间的低丰度张力。我们的模型可用于量化三轴偏倚对即将到来的星系团弱透镜巡天的宇宙学约束的影响。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Incorporating Galaxy Cluster Triaxiality in Stacked Cluster Weak Lensing Analyses
Counts of galaxy clusters offer a high-precision probe of cosmology, but control of systematic errors will determine the accuracy of this measurement. Using Buzzard simulations, we quantify one such systematic, the triaxiality distribution of clusters identified with the redMaPPer optical cluster finding algorithm, which was used in the Dark Energy Survey Year-1 (DES Y1) cluster cosmology analysis. We test whether redMaPPer selection biases the clusters’ shape and orientation and find that it only biases orientation, preferentially selecting clusters with their major axes oriented along the line of sight. Modeling the richness–mass relation as log-linear, we find that the log-richness amplitude ln (A) is boosted from the lowest to highest orientation bin with a significance of 14σ, while the orientation dependence of the richness-mass slope and intrinsic scatter is minimal. We also find that the weak lensing shear-profile ratios of cluster-associated dark halos in different orientation bins resemble a “bottleneck” shape that can be quantified with a Cauchy function. We test the correlation of orientation with two other leading systematics in cluster cosmology—miscentering and projection—and find a null correlation. The resulting mass bias predicted from our templates confirms the DES Y1 finding that triaxiality is a leading source of bias in cluster cosmology. However, the richness-dependence of the bias confirms that triaxiality does not fully resolve the tension at low-richness between DES Y1 cluster cosmology and other probes. Our model can be used for quantifying the impact of triaxiality bias on cosmological constraints for upcoming weak lensing surveys of galaxy clusters.
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